The ICMEs are identified based on inspection of a combination of signatures: an enhancement of total perpendicular pressure (Pt = B2/(2μ0) + ΣjnjkTperp,j, where j represents the three major species in the solar wind: protons, electrons and alpha particles, see Russell et al., 2005. Its gradient indicates the force), a stronger than ambient magnetic field, relatively quiet and smooth magnetic field rotations, a declining solar wind speed, a low proton temperature [Jian et al., 2006a, 2013].

At least three of the above features were required to identify an ICME. The edges of ICMEs were identified from a consensus of available features, usually delimited on sharp changes in plasma and magnetic field properties. For ambiguous events, we checked the SOHO LASCO CME catalog and STEREO SECCHI observations.

The SIRs include corotating interaction regions (CIRs) and transient stream interaction regions. The difference between a CIR and a transient SIR is only that a CIR recurs for two or more solar rotation cycles.

The SIRs are identified based on inspection of the following features: an increase of solar wind speed, a pile-up of total perpendicular pressure (Pt) with gradual decreases at both sides from the Pt peak to the edges of interaction region, velocity deflections,
a first-increase and then decrease
of proton number density, an enhancement of proton temperature,
an increase
of the entropy defined as ln(Tp3/2/Np) [Siscoe and Intriligator, 1993; Crooker et al., 1996], a compression of the magnetic field. We require the presence of at least 5 signatures, and identify SIRs with careful consideration of the ambient solar wind. For detail, please refer to Jian et al., 2006b, 2013.

The forward and reverse shocks are identified using 8-Hz magnetic field data. We rotated them into shock normal coordinates to examine the existence of associated shock waves and field changes consistent with the Rankine-Hugoniot relations. The shock normal angle (θBn), field change, and Mach number, are also given in this list.

To confirm, we have also checked the 1-min PLASTIC data. At forward shocks, all of solar wind speed, proton number density, proton temperature, and magnetic field should increase simultaneously. At reverse shocks, solar wind speed increases, while proton number density, proton temperature, and magnetic field all decrease. However, not all shocks have clear signatures in plasma properties. We indicate such shocks in the comments.